Fig. REF  shows the targets in the photometric colour-magnitude (CMD), J versus J - K\(_{\rm s}\) , plane, where J and K\(_{\rm s}\)  are VISTA photometric filters [1]}. The apparent regular distribution is caused by the photometric selection of targets in the input Gaia-ESO catalogue. For the Giraffe catalogue, the following basic selection scheme was used: \(0.00 \le (\text{J} - \text{K}_{\rm s}) \le 0.45\)  and \(14.0 \le J \le 17.5\)  for the blue box, and \(0.40 \le (\text{J} - \text{K}_{\rm s}) \le 0.70\)  and \(12.5 \le \text{J} \le 15.0\)  for the red box. The boxes were defined to maximise the probability of observing targets in all Galactic components, the discs and the halo, therefore the target densities vary drastically, and to account for this effect, the boxes were slightly extended in order to optimise the fiber occupancy in each field. In particular, in the fields, where number of targets exceeded the number of fibers - as in low latitude fields -, additional selection criteria were used, such as shifting the boxes by the mean value of extinction in a given field \(0.5\)  E(B - V). This procedure leads to a characteristic spread of the distribution along the x-axis, as seen in Fig. REF . The relative distribution is such that the majority of targets (80 \(\%\) ) are in the blue box, whereas stars in the red box account for about 20 \(\%\)  of the sample. The blue box targets include main-sequence, turnoff, and subgiant stars, and the red box was optimised for red clump stars, however because of the extension of the boxes a certain overlap exists. For the detailed description of the selection, we refer to [2]}. This selection implies that most targets in the Gaia-ESO HR10 sample are rather faint, \(14 \gtrsim \)  G\(_{\rm mag}\)  \(\lesssim 17\) , compared to other surveys such as RAVE, APOGEE, or GALAH.
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